The dynamics of the jovian magnetosphere are dominated by the mass loading of the Io torus. Sulfur dioxide and
possibly other gases such as hydrogen are sputtered from Io and are ionized. These ions in turn are accelerated by the corotational
electric field. The hot torus moves slowly outward and then ever more rapidly until reconnection releases the ions down the tail. The
outward transport is far from steady. Near Io are intense ion cyclotron waves. As observed by Galileo these waves weakened rapidly on
the side of Io closest to Jupiter. Beyond 10 Io radii (RIo) at periods less than 150s there were no discernable waves above
the instrument noise level. On the side of Io away from Jupiter the Io cyclotron waves disappeared at about 20 RIo and the
noise level in the torus reached values almost as low as those inside the Io orbit. However, as the radial distance increased so did the
noise levels. The noise levels from 0.01 to 0.1 Hz are about 2 orders of magnitude greater at 7.7 RJ than inside the Io orbit
at 5.5 RJ. The noise appears to be due to steps in the magnetic field strength and direction perhaps due to the interchange of
tubes of flux with differing plasma content. The transverse power spectral density is greater than the compressional power in this
region. The next region in which we have observations is the orbit of Europa and beyond. At frequencies of about 1 Hz the waves are more
strongly compressional than transverse in the equatorial regions and more transverse than compressional off the equator. The outer edge
of the dipolar region is about 24 RJ. The noise just inside this distance is quite variable from rotation to rotation.
Outside this distance in the magnetodisk the field crossing the current sheet varies significantly from orbit to orbit as if the
magnetodisk were globally unstable. Beyond about 40 RJ the location of the current sheet oscillates with a period of about 10
minutes. Beyond 50 RJ the plasma enters a regime of intermittent reconnection.

Introduction

Io has long been associated with disturbances in the jovian magnetosphere. Initially it was postulated that Io
conducted electric current radially in the jovian magnetosphere, currents that closed in the jovian ionosphere. These currents were in
the sense to cause JxB acceleration of the moon as if the ionosphere was attempting to accelerate Io. The currents flowing
parallel to the magnetic field were believed to become unstable, leading to potential drops that caused accelerated electrons and the
radio waves that had been observed to be controlled by Io [Bigg, 1964; Goldreich and Lynden-Bell, 1969; Piddington and Drake, 1968].

While later papers described the interaction in terms of Alfven waves [e.g. Neubauer, 1980; Southwood, et al
1980] these models retain the basic sense of a unipolar inductor generating a potential drop due to the motion of a conducting Io relative
to the magnetized plasma. Pioneer 10 and 11 revealed a magnetodisk-like magnetosphere beyond about 25 RJ . Inside this
distance the field was more dipolar. Voyager 1 and 2 were able to provide the density structure in the inner magnetosphere revealing a
hot plasma torus from about 10 RJ to 5.9 RJ, the orbit of Io . The Io interaction was speculated to produce about 1
ton/second of material . This material was ionized and quickly accelerated to corotational velocities. As this material slowly drifted
outward, currents coupling the magnetospheric plasma to the ionosphere maintained the plasma at close to corotational velocities.

Evidence for the coupling of the magnetospheric plasma to Jupiterís ionosphere comes in the form of swept back magnetic
field lines, the twist in the field associated with the field aligned current that provides the ionospheric coupling. Voyager 1 also
detected an intense current at Io . This current was limited to the near vicinity of Io and was interpreted to be the unipolar inductor
current, albeit now described as Alfven wings closing in a conducting Io. However, the mass added at Io also generates a current system.
Thus the Alfven wings may very well be generated, not by a moving conductor in a magnetized plasma, but by mass loading.

In any event the mass added to the jovian magnetosphere makes the magnetosphere a very noisy place. In this paper we
explore the activity in the magnetic field from inside the orbit of Io out to 50 RJ. These fluctuations are important because
they provide the background fluctuations in which the radiation belt particles find themselves. From the very earliest measurements
[Kivelson, 1976] it has been evident that the current sheet in the magnetodisk was much noisier than the lobes on either side and that the
compressional power was large in this region. The pre-Galileo observations have been reviewed by Khurana and Kivelson [1989], Khurana
[1993] and Glassmeier [1995]. Some of these earlier observations will be recalled as we discuss the Galileo results.

The Inner Magnetosphere

After passing by Io on December 7, 1995 the Galileo spacecraft collected magnetometer data for 30 minutes until 1815 UT
at a distance of 5.5 RJ. Telemetry was also recorded for 2 hours beginning at 2322 UT at 4.3 RJ but no attitude
data were recorded so these data are difficult to use. We will attempt to analyze herein only data for which the attitude is well
understood. The interaction with Io was extremely dynamic and is described in detail elsewhere . Ion cyclotron waves were detected
beginning about 20 RIo before Galileo passed through the wake and ceased after 10 RIo. These waves were left-hand
polarized, nearly circular, propagating nearly along the magnetic field and oscillating near the SO2+ gyrofrequency.
Amplitudes reached over 100 nT peak to peak. The wake itself was populated with mirror mode waves of even larger amplitude. These waves
were strongly compressional, and aperiodic in occurrence, with a thickness of several SO2+ ion gyroradii. We recall
that Pioneer 10 crossed the Io L shell about 52o downstream from Io and about 20 RIo off the magnetic equator.
Transverse fluctuations were observed at this location with an rms amplitude of about 10 nT [Walker and Kivelson, 1981]. Thus while the
disturbances of the plasma immediately associated with Io have a limited radial extent they do appear to extend far downstream from Io.

Once inside of 5.8 RJ the field became very quiet. This is illustrated in Figure 1 where the bottom trace
shows the transverse power (left) and the compressional power (right). Outside the orbit of Io and beyond the ion cyclotron wave region,
the wave level is also low as represented by the 1650 UT spectrum at 6.6 RJ but not quite as low as inside the Io orbit. Since
waves associated with the pitch angle scattering of particles appear to be absent in this region we expect that the plasma is stable with
respect to the ion cyclotron resonance. A possible source of free energy for wave generation is the interchange of massloaded flux tubes.
If this is true, then in the region near where this spectrum is taken the outward transport of the iogenic plasma is slightly, but not
very, unsteady, because there is very little noise in this region.

Figure 1. Power spectral density of the magnetic field obtained on the Io flyby pass on December 7, 1995 at 4
radial distances: 5.5 RJ at 1815 UT; 6.6 RJ at 1650 UT; 7.1 RJ at 1605 UT; and 7.7 RJ at 1521
UT. The compressional component is calculated from the magnitude of the magnetic field. The transverse power is the power summed over
all three vector components with the compressional power removed. The harmonic structure seen above 50 mHz in the transverse spectrum are
due to the incomplete removal of effects associated with the spin of the spacecraft in these data.

The low frequency wave amplitude increases with radial distance. Figure 1 also shows the power spectral density at
1605 UT and a radial distance of 7.1 RJ. The power continues to increase. At low frequencies the transverse power is about
equal to the compressional power. Figure 2 shows the time series corresponding to these power spectra. There is a general increase in
the level of activity, but there are also spikes seen principally in the field magnitude. We interpret these spikes as empty flux tubes
moving inward rapidly after losing their plasma in the reconnection region [Russell et al., 1998b].

Figure 2. Linearly detrended time series corresponding to the intervals over which two of the power spectra in
Figure 1 were calculated left panel) 1605 - 1615 UT; right panel) 1521-1531 UT.

The uppermost trace in Figure 1 is the power seen at 1521 UT at a radial distance of 7.7 RJ. As before the
power is similar parallel and transverse to the field. As the time series in Figure 2b shows the magnetic field consists of many
step-like disturbances. These disturbances may be due to the interchange instability . They also may be associated with the fluctuations
reported by Glassmeier et al. [1989] in this same region at slightly longer periods. Unfortunately we do not have high resolution
data on this orbit at greater radial distances. We must depend on data taken at a rate of one sample every 12 to 24 seconds and distances
greater than 10 RJ to complete our journey outward.

The Middle Magnetosphere

The jovian magnetosphere from the orbit of Europa to the inner edge of the current sheet at about 24 RJ is
the region we term the middle magnetosphere. A survey of the G2 inbound pass has been reported by Russell et al. [1998c]. We
summarize those results herein. We do not discuss the observation of an outward drifting Europa wake or inward drifting empty flux tubes
that are seen in this region as they pertain more to the circulation and dynamics of the magnetosphere that are discussed elsewhere
[Russell et al., 1998b]. Because of the telemetry limitations of the Galileo mission the data rate in the middle magnetosphere
away from the satellite encounters is generally either a sample every 12 or 24 seconds. These are frequencies generally well below the
local ion gyrofrequencies.

Figure 3 shows power spectra densities obtained at a radial distance of 10.7 RJ near and off the equator in
the left and right hand panels respectively. The compressional power and the transverse power are shown separately. The compressional
power is calculated from fast Fourier transform of the magnitude of the field. The transverse power is the total power summed over the
three sensors minus the compressional power.

Figure 3. Power spectral density of the magnetic field seen on the G2 Galileo pass at a radial distance of 10.7
RJ. The compressional and transverse power are shown separately. a) Spectra obtained from 1440-1545 UT on September 7, 1996
near the magnetic equator. b) Spectra obtained from 1145-1345 UT at the highest magnetic latitudes reached by Galileo (Russell et al.,
1998c).

The compressional power and the transverse power vary with latitude out of phase. The compressional power is strongest
near the equator and weakest at high latitudes. The transverse power is greater at high latitudes than at low latitudes. Near the
equator the compressional power is greater than the transverse power below about 5 mHz otherwise the transverse power usually dominates in
this region. At high latitudes there is little compressional power at any frequency.

Further out in the magnetosphere where the magnetodisk current layer is beginning to form, the fluctuations at the
current layer crossing are more isotropic across the entire frequency band so that the compressional and transverse powers are nearly
equal and about an order of magnitude greater than the total power seen in Figure 3. This is illustrated with the top spectra of Figure 4
for a current sheet crossing at 23 RJ. In contrast in this region off the equator the wave spectrum is very quiet. This is
shown with the lower spectra of Figure 4 taken at 25 RJ where the waves are about a factor of 200 lower in power than spectra
at the equator.

In summary the wave power in the middle magnetosphere is strong but not as strong as in the outer part of the torus.
Near the equator the waves are much more strongly compressional than off the equator, and in the outer part of the inner magnetosphere, or
more properly above and below the inner part of the magnetodisk even the transverse waves are weak.

Figure 4. Power spectral density of the magnetic field seen at the inner edge of the magnetodisk on the G2
inbound pass at radial distances of 23 and 25 RJ. (Top) Measurements crossing the current sheet from 2100 to 2205 UT September
5, 1996. (Bottom) Measurements obtained in the lobes away from the current sheet crossing over the period 1700 to 1900 UT (Russell et
al., 1998c).

TRANSIENT EVENTS IN THE OUTER MIDDLE MAGNETOSPHERE

On the G2 inbound pass there was a gradual transition of wave properties with radial distance. This was not true on
G1. As the spacecraft crossed into the quasi dipolar region of the magnetosphere near 24 RJ and left the magnetodisk the
magnetic field became very disturbed for an entire rotation [Russell et al., 1998d]. The time series for this period is shown in
Figure 5a where the data have been high pass filtered with a corner frequency of 0.75 mHz. The waveforms are quite irregular even spiky
in appearance. This disturbance lasted an entire rotation and then became much quieter as illustrated in the next rotation of the planet
shown in Figure 5b. Because the disturbance lasted an entire rotation it must have been global in nature. Figure 6 contrasts the noise
seen during these two successive rotations beginning at 0830 UT and 2130 UT on June 26, 1996. At lowest frequencies the power is enhanced
a factor of 10 in both the transverse and compressional power and a factor of 3 at the highest frequencies. During both intervals, the
power falls off more rapidly in the compressional component than the transverse so that at highest frequencies (here 20 mHz), the waves
are mainly transverse.

Figure 5. High pass filtered magnetic field observations in the outer portion of the middle magnetosphere on the G1
inboard pass during a disturbed period. a) the period 0830 to 1715 on June 26, 1996 b) the period 2130 of June 26 to 0545 of June 27,
1996, the jovian rotation immediately following the first interval. The periods are not exactly contiguous because of a data
gap.

The Magnetodisk

The transient disturbance in the outer part of the middle magnetosphere is our first clue that the magnetosphere can
change from day to day. We also have evidence for this in the variability of the component of the magnetic field that crosses the current
sheet. This variability has been discussed by Russell et al. [1998d]. The cross product of this component and the current is a
measure of the magnetic force on the plasma, the curvature and pressure forces. We can estimate the current density from the change in
the radial component of the magnetic field across the current sheet. The magnetic force as a function of radius, calculated at each
current sheet crossing is shown in Figure 7. While the magnetic stress in the middle magnetosphere is relatively constant from pass to
pass the stress beyond 24 RJ in the magnetodisk is quite varied from pass to pass.

Figure 6. Compressional and transverse power spectral densities corresponding to the time intervals
in Fig. 5.

Figure 7. Magnetic stress integrated across the current sheet for the first 4 inbound Galileo
passes as a function of radial distance (Russell et al., 1998d).

We can carry this analysis one step further by estimating the pressure in the current sheet and how it varies with
radial distance. Since the three principal forces on the plasma are the magnetic force, the particle pressure force and the centrifugal
force, we can estimate the centrifugal force from these other two forces assuming they are in balance. If we assume further that the
plasma is rotating with the same period as Jupiter, then we can calculate the mass density from the centrifugal force. This has been done
by Russell et al. [1998d] and they find that the radial fall off in plasma density is generally quite smooth except for one of the
orbits G2 when the density appeared to drop to lower levels. This could indicate that there is variation in the density profile or that
one of our assumptions is incorrect on this orbit. Since the iogenic heavy ions must be carried radially outward in the magnetosphere,
this declining radial density profile can be used to calculate a radial velocity profile. This has been done by Russell et al.
[1998b], who find that the velocity rises from a few m/s at Io to about 50 km/s at 40 RJ.

Two changes occur in the fluctuations associated with the current sheet as one proceeds outward. First, the strength
of the "turbulence" in the current sheet increases relative to the strength of the normal component crossing the sheet. In the
inner part of the magnetodisk the turbulence is sufficiently small that it does not result in reversals of the magnetic field component
crossing the sheet. However, at about 45 RJ and beyond this distance the normal component begins to reverse suggesting that
there is tearing occurring in the current sheet [Russell et al., 1998e; 1998f]. It is conjectured that the growth of these tearing
islands, allowing low density regions above and below the current sheet to become connected, leads to explosive reconnection of the
magnetodisk lobes and the formation of magnetized islands of heavy ions that are ejected from the magnetosphere down the tail. We discuss
this process briefly in the next section.

A second persistent fluctuation in the magnetodisk is a "10-minute" oscillation in its position. This is in
addition to the motion of the warped current sheet in synchronism with the planetary rotation. The amplitude of this 10 minute wave is
greatest at largest radial distances resulting in multiple crossings of the current sheet [Russell et al., 1998e]. This wave is
possibly the same phenomenon as seen by Voyager 2 in the magnetodisk region and interpreted as a standing Alfven wave [Khurana and
Kivelson, 1989].

The Near Tail Region and the Formation of Empty Flux Tubes

The magnetospheric magnetic field is ultimately rooted in the planetary interior. The number of field lines exiting
the surface of the planet is fixed and on the time scale of the dynamics of the jovian magnetosphere their location is quite fixed as
well. Io keeps adding plasma to the magnetosphere and as we have seen above there is much evidence that it moves slowly outward carrying
magnetic flux with it. The magnetosphere cannot lose magnetic field lines threading the surface but it must ultimately lose the ions.
Thus there must be a mechanism that separates the magnetic field from the ions and allows the ions to escape from Jupiter. Vasyliunas
[1983] proposed a circulation model in which a steady state reconnection line formed across the tail that separated the ion laden ends of
the field from the less densely populated inner parts of the field lines. The G8 pass of Galileo through this region allows us to
determine if this strongly non-linear process occurs.

Figure 8. Magnetic field in the radial, south, tangential (rst) coordinate system as Galileo proceeded from 100
RJ to 50 RJ and from midnight to 0300 LT on the G8 orbit

Figure 8 shows the magnetic field measured by Galileo in the rst coordinate system where r is radially outward, s is
southward and t is tangential to the corotational flow direction for the region from 100 RJ to 50 RJ and midnight to
0300 LT. The large "sine" wave in Br and Bt is the field reversal associated with crossing the
magnetotail current sheet. The minor component of the magnetic field Bs appears to have a number of "glitches".
These glitches are real and last up to an hour in length and represent reconnection, localized in space and time occurring beyond 50
RJ (Russell et al., 1998f,g). The large size of the reconnected normal component indicates the explosive or rapid
nature of this process. So while the moon Io provides the ultimate source of energy through the mass loading process, transient
reconnection is the process that dynamically releases this energy in the outer magnetosphere.

In addition to leading to a reconfiguration of the magnetic field, the reconnection process creates "empty"
buoyant regions whose centrifugal force is much less than that of the unreconnected field. These tubes must interchange with the full
field lines to get back to the orbit of Io and repeat the convection cycle. From observations in the middle (Russell et al.,
1998c) and inner magnetosphere (Russell et al., 1998b) it appears that the way this process occurs is through the generation of
small tubes that can move rapidly through the more slowly moving outward flux. These tubes contain less plasma and hence have higher
field strengths than the ion laden flux tubes. Thus they can be detected if the telemetry rate is sufficiently high. To date
"empty" tubes have been detected but their size is close to the limits of detectability (Russell et al., 1998b).

Summary and Conclusions

The mass loading at Io sets in motion a large circulation system that begins in the Io torus, transports ions and
magnetic flux to the near tail region and then returns the magnetic flux to the inner magnetosphere. This circulation process is unsteady
as indicated by the variation seen in the magnetic stresses in the magnetodisk [Russell et al, 1998 b, d]. Inside the orbit of Io
the magnetosphere is relatively quiet at frequencies from 5 mHz to 2 Hz. Outside of Io the noise increases with radial distance to at
least 7 RJ. This noise is in part due to step functions in the field strength that suggest that flux tube interchange is
occurring. While the middle magnetosphere is not much noisier than the outer torus magnetosphere, the nature of the fluctuation appears
to change with the radial distance beyond the orbit of Europa. Close to the equator the fluctuations are fairly isotropic with roughly
equal power in the compressional and transverse waves while at high latitudes the waves are largely transverse to the field. In the
magnetodisk region the high latitude magnetosphere is very quiet while the current sheet remains noisy. The strength of this noise
increases with radial distance until at about 50 RJ the reversals in the normal component associated with the turbulence become
large enough to initiate explosive reconnection across the current sheet. This is not the only "global" instability in the
magnetosphere. The properties of the magnetodisk do vary from pass to pass especially the normal component of across the current sheet.
On one pass the region of the outer middle magnetosphere became disturbed for an entire rotation of the planet. Finally in addition to
the motion of the warped current sheet at the planetary rotation period, the current sheet moves up and down with an approximate 10 minute
period. It is not clear what causes this fluctuation, dynamics in the inner regions or the outer regions but its amplitude is clearly
larger at greater radial distances.

Overall we can ascribe most of the fluctuations in the jovian magnetosphere within about 100 RJ to endogenic
sources. This is not to say that we cannot detect the influences of the solar wind on the system. The solar wind clearly sets the
geometry of the tail region. When the solar wind has a northerly flow the tail current is lifted northward above the equatorial plane in
which Galileo orbits. When the solar wind dynamic pressure is high, the field strength in the lobes is enhanced. It is possible even
that disturbances in the solar wind could trigger disturbances in the outer magnetodisk. However, thus far it is possible to ascribe all
the transient disturbances that we see to processes originating within the magnetosphere itself.

Acknowledgments

This work was supported by the National Aeronautics and Space Administration through a grant administered by the
Jet Propulsion Laboratories.